Ultradeep Near-Infrared ISAAC Observations of the Hubble Deep Field South: Observations, Reduction, Multicolor Catalog, and Photometric Redshifts

By I. Labbé, M. Franx, G. Rudnick, N. F. Förster Schreiber, Hans-Walter Rix, A. Moorwood, P. V. van Dokkum, P. P. van der Werf, H. Röttgering, L. van Starkenburg and 3 more. 2002

216 citations recorded by the source corpus.

We present deep near-infrared (NIR) Js-, H-, and Ks-band ISAAC imaging of the Wide Field Planetary Camera 2 (WFPC2) field of the Hubble Deep Field South (HDF-S). The 2.′5 × 2.′5 high Galactic latitude field was observed with the Very Large Telescope under the best seeing conditions, with integration times amounting to 33.6 hr in Js, 32.3 hr in H, and 35.6 hr in Ks. We reach total AB magnitudes for point sources of 26.8, 26.2, and 26.2, respectively (3 σ), which make it the deepest ground-based NIR observation to date and the deepest Ks-band data in any field. The effective seeing of the co-added images is ≈0.″45 in Js, ≈0.″48 in H, and ≈0.″46 in Ks. Using published WFPC2 optical data, we constructed a Ks-limited multicolor catalog containing 833 sources down to K ≲ 26, of which 624 have seven-band optical-to-NIR photometry. These data allow us to select normal galaxies from their rest-frame optical properties to high redshift (z ≲ 4). The observations, data reduction, and properties of the final images are discussed, and we address the detection and photometry procedures that were used in making the catalog. In addition, we present deep number counts, color distributions, and photometric redshifts of the HDF-S galaxies. We find that our faint Ks-band number counts are flatter than published counts in other deep fields, which might reflect cosmic variations or different analysis techniques. Compared to the HDF-N, we find many galaxies with very red V-H colors at photometric redshifts 1.95 < zphot < 3.5. These galaxies are bright in Ks, with infrared colors redder than Js-Ks > 2.3 (in Johnson magnitudes). Because they are extremely faint in the observed optical, they would be missed by ultraviolet–optical selection techniques, such as the U-dropout method.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/68b561fa1c7b3d34caaba709c7926eb3a7a1eefc

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Citations in the corpus

EAZY: A Fast, Public Photometric Redshift Code (2008, unknown): “∼5 UBV IJHK ∼24 Fernández-Soto, Lanzetta, & Yahil (1999) HDF-S . . . . . . . . 4.5 UBV IJHK + IRAC 26.2 Labbé et al. (2003) MS-1054 . . . . . .”
CEERS Epoch 1 NIRCam Imaging: Reduction Methods and Simulations Enabling Early JWST Science Results (2022, methodology): “In this case, the noise in the resampled science images and variance maps is reduced by the cor- relations, and so photometric uncertainties will by underestimated (e.g., Casertano et al. 2000; Labbé et al. 2003; Blanc et al. 2008; Whitaker et al. 2011; Papovich et al. 2016).”
3D-HST WFC3-SELECTED PHOTOMETRIC CATALOGS IN THE FIVE CANDELS/3D-HST FIELDS: PHOTOMETRY, PHOTOMETRIC REDSHIFTS, AND STELLAR MASSES (2014, methodology): “This method, described in more detail in Labbé et al. (2003), closely approximates the methodology that is used for the actual flux measurements and is insensitive to noise correlations (which affect error estimates based on the observed pixel-to-pixel variation, such as the errors that are…”
What Do We Learn from IRAC Observations of Galaxies at 2 < z < 3.5? (2006, methodology): “′′2396 pixel scale) version of an existing ISAAC K-band image (Labbé et al. 2003, hereafter L03)1, and average-combined.”
The Multiwavelength Survey by Yale-Chile (MUSYC): Survey Design and Deep Public UBVRIz' Images and Catalogs of the Extended Hubble Deep Field-South (2005, methodology): “An alternative formula suggested by Labbé et al. (2003), σN = σ1aN+σ1bN2 , (5) yields an equally good fit, witha = 1.007,b = 0.051.”
Stellar Population Diagnostics of Elliptical Galaxy Formation (2006, methodology): “Finally, the HDF-South optical data were complemented by ultra-deep JHK imaging at the VLT (the FIRES survey, Labbé et al. 2003, Franx et al. 2003), revealing a population of near-IR galaxies with very red colors (J −K > 2.3), called distant red galaxies (DRG), a fraction of which may be ETGs at…”
SWIRE: The SIRTF Wide‐Area Infrared Extragalactic Survey (2001, background): “On the other hand, Benson et al. (2001) find that hierarchical models under-predict the proportion of high-redshift, homogeneous, passively evolving objects, and Labbe et al. (2003) find a much larger population of red systems with zphot >2 in the HDF-S than Dickinson et al. (2003) do in HDF-N.”
AN ULTRA-DEEP NEAR-INFRARED SPECTRUM OF A COMPACT QUIESCENT GALAXY AT z = 2.2 (2009, background): “Due to the introduction of large photometric surveys with deep NIR imaging (e.g., Labbé et al. 2003; Franx et al. 2003), many quiescent massive galaxies beyond z = 2 have been identified in the past few years (e.g., Förster Schreiber et al. 2004; Daddi et al. 2004a,b; Labbé et al. 2005).”
A PUBLIC Ks-SELECTED CATALOG IN THE COSMOS/UltraVISTA FIELD: PHOTOMETRY, PHOTOMETRIC REDSHIFTS, AND STELLAR POPULATION PARAMETERS, (2013, methodology): “…galaxies (e.g., Franx et al. 2003; Förster Schreiber et al. 2004; Daddi et al. 2005; van Dokkum et al. 2006) such as FIRES (0.002 deg2, Labbé et al. 2003), GOODS (0.04 deg2, Wuyts et al. 2008) and MUSYC (Quadri et al. 2007, 0.12 deg2), have now been superceded by much wider surveys…”